arxiv: 2604.22605 · v1 · submitted 2026-04-24 · 🌌 astro-ph.SR · astro-ph.HE· hep-ph· nucl-th

Recognition: unknown

The Effect of Mass Loss and Convective Overshooting on the Pre-Collapse Structure, Composition, and Neutrino Emission of Red Supergiants

McKenzie A. Myers , Claire B. Campbell , Kelly M. Patton , Segen BenZvi , Marta Colomer Molla , Alec Habig , James P. Kneller , Dan Milisavljevic

show 1 more author

Jeffrey Tseng

Authors on Pith no claims yet

Pith reviewed 2026-05-08 09:46 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HEhep-phnucl-th

keywords red supergiantspre-supernova neutrinosstellar evolutionmass lossconvective overshootingcore collapseneutrino emission

0 comments

The pith

Mass loss and convective overshooting alter red supergiant core evolution, causing pre-supernova neutrino emission to shift to higher energies and become beta-process dominated hours before collapse.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper investigates the impact of different mass-loss rates and convective overshooting treatments on the structure, composition, and neutrino output of red supergiants in the final stages leading to core collapse. Using a series of stellar models, it demonstrates that the core contracts and heats while deleptonizing, but silicon burning episodes interrupt this with expansion and mixing. These internal changes produce a detectable evolution in the neutrino signal, with increasing energy and flux that shifts to beta-decay dominance close to explosion. Such signals from a nearby star could provide advance information on an impending supernova.

Core claim

Models of red supergiants show that in the last days before collapse the core contracts, heats, and deleptonizes, but core silicon burning and shell burning cause temporary expansion and convective mixing with higher-proton-fraction material; the resulting pre-SN neutrino emission shifts gradually to higher energies and larger flux, becoming dominated by beta processes a few hours prior to collapse.

What carries the argument

A grid of MESA models with 12-20 solar mass zero-age main sequence stars, Dutch mass-loss scheme at efficiencies 0.2-1.0, two convective overshooting schemes, and a 206-isotope network that tracks composition to compute neutrino emission from the evolving core.

If this is right

The timing of the neutrino flux increase depends on when silicon burning initiates in the core.
Convective mixing during shell burning temporarily reverses deleptonization, affecting the neutrino spectrum.
Stars with higher mass-loss rates evolve differently in core composition, leading to varied neutrino signals.
The shift to beta-process dominance provides a temporal marker for the final hours before collapse.
Pre-SN neutrinos from RSGs within 1 kpc become observable with current detectors due to the increased flux.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

Observing the neutrino spectrum evolution could constrain the uncertain mass-loss rates in massive stars.
Similar modeling for other progenitor types might reveal distinct pre-SN neutrino signatures.
Combining neutrino data with electromagnetic observations of the progenitor could test stellar evolution assumptions.
The findings suggest that pre-collapse neutrino monitoring could give hours of warning for nearby supernovae.

Load-bearing premise

The chosen Dutch mass-loss scheme, specific overshooting parameters, and 206-isotope network in MESA capture the dominant physics of red supergiant core evolution without large systematic errors from missing processes.

What would settle it

A detected pre-collapse neutrino signal from a nearby red supergiant whose energy spectrum and flux evolution do not match the predicted gradual increase and beta-process dominance in the final hours.

Figures

Figures reproduced from arXiv: 2604.22605 by Alec Habig, Claire B. Campbell, Dan Milisavljevic, James P. Kneller, Jeffrey Tseng, Kelly M. Patton, Marta Colomer Molla, McKenzie A. Myers, Segen BenZvi.

**Figure 1.** Figure 1: FIG. 1. The evolution of the luminosity and effective surface view at source ↗

**Figure 2.** Figure 2: FIG. 2. The luminosity and effective surface temperature of view at source ↗

**Figure 3.** Figure 3: FIG. 3. The evolution of the luminosity and effective surface view at source ↗

**Figure 5.** Figure 5: FIG. 5. The evolution of the central temperature and density view at source ↗

**Figure 6.** Figure 6: FIG. 6. The compactness view at source ↗

**Figure 7.** Figure 7: FIG. 7. The compactness view at source ↗

**Figure 9.** Figure 9: FIG. 9. The convective regions (top panel), core electron frac view at source ↗

**Figure 10.** Figure 10: FIG. 10. The core mass fraction of ten selected isotopes for all models. For each isotope, the symbols shifted leftwards indicate view at source ↗

**Figure 11.** Figure 11: FIG. 11. The total neutrino emission spectra, including both beta and pair processes, for all of the RSG models. The earliest view at source ↗

**Figure 12.** Figure 12: FIG. 12. The total neutrino luminosity, beta and pair processes combined, as a function of time for all RSG models. view at source ↗

read the original abstract

Prior to core collapse, the neutrino emission from red supergiants (RSGs) is so large that a nearby ($\lesssim1$kpc) RSG will become visible in current and near-future neutrino detectors. The rate of emission and the spectra of the pre-supernova (pre-SN) neutrinos from RSGs are sensitive to the temperature, density, and detailed isotopic composition of the core. During the last year of the star's life, these properties change considerably. Several factors of stellar evolution modeling - such as the treatment of mass loss and convective overshooting - alter the thermal conditions and composition of the RSG core as it approaches collapse. In this paper we present the first study of how varying the treatment of mass loss and convective overshooting together affects the pre-collapse core properties and neutrino emission of RSGs. We use the stellar evolution instrument MESA and construct a grid of 32 models with zero-age main sequence masses of $\{ 12, 15, 18, 20\}$ $M_\odot$, use the so-called 'Dutch' mass-loss scheme with wind efficiencies of $\{0.2, 0.4, 0.8, 1.0\}$, and consider two convective overshooting schemes. Our models use a large 206-isotope nuclear network in order to accurately compute the structure and composition of the star. We find that, in the last few days of the star's life, the general trend of the conditions and composition in the core of the star is one of contraction, heating, and deleptonization, but that during this phase, this general trend will be interrupted by the initiation of core silicon burning and shell burning episodes that cause the core to expand and undergo convective mixing with material of a higher proton fraction that temporarily reverses the deleptonization. The pre-SN neutrino emission reflects these changes with a gradual shift to higher energies and larger flux that becomes dominated by beta processes a few hours prior to the collapse.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

This MESA grid shows mass loss and overshooting shift pre-SN neutrino energies and flux in RSGs, with beta processes taking over hours before collapse, but the trends rest on unvalidated Dutch wind and overshooting choices.

read the letter

The main takeaway is that this paper runs 32 MESA models varying ZAMS mass, Dutch wind efficiency, and two overshooting schemes to track how those choices alter core contraction, silicon burning episodes, and the resulting neutrino emission in the final days. It is the first explicit combination of both parameters on pre-collapse neutrinos with a 206-isotope network, and that is the concrete addition over earlier single-parameter runs. The models show the expected overall contraction and deleptonization interrupted by shell burning and mixing, which produces a gradual rise in neutrino energy and flux that flips to beta-process dominance a few hours out. That qualitative pattern is useful for people planning nearby RSG neutrino searches. The calculations are straightforward to reproduce in MESA, and the large network is a plus for composition accuracy. The soft spots are the lack of any cross-code checks or observational anchors for the core state at collapse, plus no reported error bars or sensitivity tests on the wind efficiencies. The Dutch scheme and overshooting parameters are known to be tunable and uncertain; if they mis-time the silicon burning relative to reality, the reported few-hour window and energy shift can move. The trends are presented as general but come from one code family without external falsification. This work is aimed at neutrino observers and supernova modelers who need to understand parameter sensitivities in pre-SN signals. A reader already using MESA or working on detector strategies will get practical numbers to compare against. It is solid enough on its own terms to deserve referee time rather than a desk reject, even though revisions will likely be needed for quantitative uncertainties and validation.

Referee Report

2 major / 2 minor

Summary. The manuscript constructs a grid of 32 MESA models of red supergiants (ZAMS masses 12–20 M⊙) that vary the Dutch wind efficiency factor (0.2–1.0) and employ two convective overshooting prescriptions while using a 206-isotope network. It reports that the final days of evolution are characterized by core contraction, heating, and deleptonization, interrupted by silicon burning and shell-burning episodes that drive expansion and mixing; these structural changes produce a gradual increase in pre-SN neutrino flux and mean energy, with beta processes becoming dominant a few hours before collapse.

Significance. If the reported trends are robust within the adopted physics, the work supplies the first systematic exploration of the joint effect of mass-loss efficiency and overshooting on pre-collapse neutrino emission from RSGs. The use of an extended nuclear network and an explicit 32-model grid are strengths that allow direct assessment of parameter sensitivity; the results bear on the expected signal in near-future neutrino detectors for a Galactic supernova progenitor.

major comments (2)

[Abstract and §4] Abstract and §4: The central claim that beta processes dominate the neutrino emission 'a few hours prior to collapse' is load-bearing for the neutrino-emission conclusion, yet the manuscript provides no quantitative definition of dominance (e.g., fractional contribution threshold) nor shows the time-dependent breakdown of emission channels for representative models across the grid. Without this, it is unclear how sensitive the reported few-hour window is to the precise timing of Si burning.
[§3.1 and Table 1] §3.1 and Table 1: The Dutch wind efficiencies and the two overshooting schemes are varied explicitly, but the paper does not quantify how the resulting core-mass and mixing differences propagate into the exact onset time of core Si burning or the duration of the beta-dominated phase. A sensitivity plot or table showing the spread in these timings across the 32 models would be required to substantiate that the qualitative trend is not an artifact of the particular parameter choices.

minor comments (2)

[§2] The abstract states that the models use a 'large 206-isotope nuclear network' but does not specify which reactions are included or omitted for the weak processes that dominate the late-time neutrino emission; a brief statement in §2 would improve reproducibility.
[Figures] Figure captions and axis labels in the neutrino-related figures should explicitly state the energy range and the definition of 'mean energy' used, as these quantities are central to the reported spectral shift.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. The comments highlight areas where additional clarity and quantification will strengthen the presentation of our results on pre-collapse neutrino emission. We address each major comment below and will revise the manuscript accordingly.

read point-by-point responses

Referee: [Abstract and §4] Abstract and §4: The central claim that beta processes dominate the neutrino emission 'a few hours prior to collapse' is load-bearing for the neutrino-emission conclusion, yet the manuscript provides no quantitative definition of dominance (e.g., fractional contribution threshold) nor shows the time-dependent breakdown of emission channels for representative models across the grid. Without this, it is unclear how sensitive the reported few-hour window is to the precise timing of Si burning.

Authors: We agree that a precise definition and explicit channel breakdown would improve the robustness of this key claim. In the revised manuscript we will define 'dominance' quantitatively as the epoch when beta-process neutrinos exceed 50% of the total neutrino luminosity. We will add a new figure in §4 showing the time-dependent fractional contributions from beta, pair, and other processes for at least four representative models spanning the grid (different masses and wind efficiencies). The figure will also mark the onset of core Si burning to illustrate the sensitivity of the few-hour window. These additions will make the reported trend directly verifiable from the data. revision: yes
Referee: [§3.1 and Table 1] §3.1 and Table 1: The Dutch wind efficiencies and the two overshooting schemes are varied explicitly, but the paper does not quantify how the resulting core-mass and mixing differences propagate into the exact onset time of core Si burning or the duration of the beta-dominated phase. A sensitivity plot or table showing the spread in these timings across the 32 models would be required to substantiate that the qualitative trend is not an artifact of the particular parameter choices.

Authors: We concur that quantifying the spread in Si-burning onset and beta-phase duration across the full grid is necessary to demonstrate that the reported behavior is not sensitive to specific parameter choices. In the revision we will insert a new table in §3.1 (or an accompanying figure) that reports, for every model, (i) the time from core Si ignition to collapse and (ii) the duration of the beta-dominated neutrino phase. The table will be accompanied by a brief discussion of trends with Dutch wind efficiency and overshooting scheme. This will directly address the propagation of core-mass and mixing differences into the neutrino-emission timeline. revision: yes

Circularity Check

0 steps flagged

No significant circularity in forward simulation results

full rationale

The paper constructs a grid of 32 MESA models varying ZAMS mass, Dutch wind efficiencies, and two overshooting schemes, then directly evolves each model with a 206-isotope network to obtain core temperature-density-composition histories and the resulting neutrino spectra. All reported trends (core contraction/heating/deleptonization interrupted by Si burning, gradual neutrino energy/flux shift, and late beta-process dominance) are numerical outputs of these simulations rather than any analytical derivation, fitted parameter renamed as prediction, or self-citation chain. No load-bearing premise reduces to its own inputs by construction, and the analysis remains self-contained against the stated modeling choices.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central findings rest on the validity of MESA's implementation of the Dutch wind prescription and the two overshooting schemes, plus the assumption that a 206-isotope network suffices for core composition tracking. No new entities are postulated.

free parameters (2)

wind efficiency factor
Explicitly varied over {0.2, 0.4, 0.8, 1.0} in the Dutch scheme; chosen by hand for the grid rather than fitted to data.
convective overshooting parameters
Two distinct schemes considered; specific numerical values not stated in abstract but treated as variable inputs.

axioms (2)

domain assumption MESA stellar evolution code accurately models RSG structure and evolution under the chosen physics inputs
Invoked throughout the grid construction and core property tracking described in the abstract.
domain assumption The 206-isotope nuclear network provides sufficient accuracy for isotopic composition and neutrino-producing reactions
Stated as necessary to compute structure and composition accurately.

pith-pipeline@v0.9.0 · 5733 in / 1539 out tokens · 36920 ms · 2026-05-08T09:46:40.638875+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

84 extracted references · 53 canonical work pages · 2 internal anchors

[1]

core only

assumes that mass-loss rates depend most heavily on luminosity and effective temperature, some more re- cent studies propose that it is the wind profile density distribution that most strongly affects mass-loss rates [20]. Others have found evidence supporting the idea that mass-loss rates are strongly related to the convec- tive velocity of RSG chromosph...
[2]

compactness

[64]. As equation (6) indicates, the beta neutrino emission is proportional to the density, and the thermal neutrinos are also functions ofρandTvia the distribu- tions of the electron-positron momenta in equation (7). Thus, the differences in the mass loss and overshooting treatment will affect the pre-SN neutrino emission start- ing with carbon burning, ...
[3]

E. M. Levesque,Astrophysics of Red Supergiants, 2514- 3433 (IOP Publishing, 2017)

2017
[4]

Davies, Red supergiants as supernova progenitors, Philosophical Transactions of the Royal Society of Lon- don Series A375, 20160270 (2017)

B. Davies, Red supergiants as supernova progenitors, Philosophical Transactions of the Royal Society of Lon- don Series A375, 20160270 (2017)

2017
[5]

S. D. Van Dyk, Red Supergiants as Supernova Progen- itors, Galaxies13, 33 (2025), arXiv:2507.15973 [astro- ph.SR]

work page arXiv 2025
[6]

Habig and K

A. Habig and K. Scholberg, The Supernova Early Warn- ing System, Nature Reviews Physics2, 458 (2020)

2020
[7]

Al Kharusi, S

S. Al Kharusi, S. Y. BenZvi, J. S. Bobowski, W. Bonivento, V. Brdar, T. Brunner, E. Caden, M. Clark, A. Coleiro, M. Colomer-Molla, J. I. Crespo- Anad´ on, A. Depoian, D. Dornic, V. Fischer, D. Franco, W. Fulgione, A. Gallo Rosso, M. Geske, S. Gris- wold, M. Gromov, D. Haggard, A. Habig, O. Halim, A. Higuera, R. Hill, S. Horiuchi, K. Ishidoshiro, C. Kato, ...

work page arXiv 2021
[8]

M. Kara, S. Torres-Lara, A. L. Baxter, S. BenZvi, M. Colomer Molla, A. Habig, J. P. Kneller, M. Lai, R. F. Lang, M. Linvill, D. Milisavljevic, J. Migenda, C. Orr, K. Scholberg, J. Smolsky, J. Tseng, C. D. Tun- nell, J. Vasel, and A. Sheshukov, The SNEWS 2.0 alert software for the coincident detection of neutrinos from core-collapse supernovae, Journal of ...

work page arXiv
[9]

Healy, S

S. Healy, S. Horiuchi, M. Colomer Molla, D. Milisavl- jevic, J. Tseng, F. Bergin, K. Weil, M. Tanaka, and S. Otero, Red supergiant candidates for multimessenger monitoring of the next Galactic supernova, MNRAS529, 3630 (2024), arXiv:2307.08785 [astro-ph.SR]

work page arXiv 2024
[10]

Beaudet, V

G. Beaudet, V. Petrosian, and E. E. Salpeter, Energy Losses due to Neutrino Processes, ApJ150, 979 (1967)

1967
[11]

N. Itoh, H. Hayashi, A. Nishikawa, and Y. Kohyama, Neutrino Energy Loss in Stellar Interiors. VII. Pair, Photo-, Plasma, Bremsstrahlung, and Recombination Neutrino Processes, Astrophysical Journals102, 411 (1996)

1996
[12]

Farag, F

E. Farag, F. X. Timmes, M. Taylor, K. M. Patton, and R. Farmer, On stellar evolution in a neutrino 15 hertzsprung–russell diagram, The Astrophysical Journal 893, 133 (2020)

2020
[13]

S. E. Woosley, A. Heger, and T. A. Weaver, The evolution and explosion of massive stars, Rev. Mod. Phys.74, 1015 (2002)

2002
[14]

Odrzywolek, M

A. Odrzywolek, M. Misiaszek, and M. Kutschera, Detec- tion possibility of the pair-annihilation neutrinos from the neutrino-cooled pre-supernova star, Astroparticle Physics21, 303 (2004)

2004
[15]

Asakura, A

K. Asakura, A. Gando, Y. Gando, T. Hachiya, S. Hayashida, H. Ikeda, K. Inoue, K. Ishidoshiro, T. Ishikawa, S. Ishio, M. Koga, S. Matsuda, T. Mitsui, D. Motoki, K. Nakamura, S. Obara, T. Oura, I. Shimizu, Y. Shirahata, J. Shirai, A. Suzuki, H. Tachibana, K. Tamae, K. Ueshima, H. Watanabe, B. D. Xu, A. Ko- zlov, Y. Takemoto, S. Yoshida, K. Fushimi, A. Piepk...

work page arXiv 2016
[16]

Guo, Y.-Z

G. Guo, Y.-Z. Qian, and A. Heger, Presupernova neu- trino signals as potential probes of neutrino mass hierar- chy, Physics Letters B796, 126 (2019), arXiv:1906.06839 [astro-ph.HE]

work page arXiv 2019
[17]

C. Kato, K. Ishidoshiro, and T. Yoshida, Theoretical Pre- diction of Presupernova Neutrinos and Their Detection, Annual Review of Nuclear and Particle Science70, 121 (2020), arXiv:2006.02519 [astro-ph.HE]

work page arXiv 2020
[18]

Mukhopadhyay, C

M. Mukhopadhyay, C. Lunardini, F. X. Timmes, and K. Zuber, Presupernova Neutrinos: Directional Sensitiv- ity and Prospects for Progenitor Identification, ApJ899, 153 (2020), arXiv:2004.02045 [astro-ph.HE]

work page arXiv 2020
[19]

S. Abe, M. Eizuka, S. Futagi, A. Gando, Y. Gando, S. Goto, T. Hachiya, K. Hata, K. Ichimura, S. Ieki, H. Ikeda, K. Inoue, K. Ishidoshiro, Y. Kamei, N. Kawada, Y. Kishimoto, M. Koga, M. Kurasawa, T. Mitsui, H. Miyake, D. Morita, T. Nakahata, R. Nakajima, K. Nakamura, R. Nakamura, R. Nakamura, J. Nakane, H. Ozaki, K. Saito, T. Sakai, I. Shimizu, J. Shirai, ...

work page arXiv 2024
[20]

Meynet, V

G. Meynet, V. Chomienne, S. Ekstr¨ om, C. Georgy, A. Granada, J. Groh, A. Maeder, P. Eggenberger, E. Levesque, and P. Massey, Impact of mass-loss on the evolution and pre-supernova properties of red super- giants, A&A575, A60 (2015), arXiv:1410.8721 [astro- ph.SR]

work page arXiv 2015
[21]

Renzo, C

M. Renzo, C. D. Ott, S. N. Shore, and S. E. de Mink, Sys- tematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars, A&A603, A118 (2017), arXiv:1703.09705 [astro-ph.SR]

work page arXiv 2017
[22]

Antoniadis, A

K. Antoniadis, A. Z. Bonanos, S. de Wit, E. Za- partas, G. Munoz-Sanchez, and G. Maravelias, Estab- lishing a mass-loss rate relation for red supergiants in the Large Magellanic Cloud, A&A686, A88 (2024), arXiv:2401.15163 [astro-ph.SR]

work page arXiv 2024
[23]

Fuller and D

J. Fuller and D. Tsuna, Boil-off of red supergiants: mass loss and type II-P supernovae, The Open Journal of As- trophysics7, 47 (2024), arXiv:2405.21049 [astro-ph.SR]

work page arXiv 2024
[24]

Antoniadis, E

K. Antoniadis, E. Zapartas, A. Z. Bonanos, G. Mar- avelias, S. Vlassis, G. Mu˜ noz-Sanchez, C. Nally, M. Meixner, O. C. Jones, L. Lenki´ c, and P. J. Kavanagh, Investigating the metallicity dependence of the mass-loss rate relation of red supergiants, A&A702, A178 (2025), arXiv:2503.05876 [astro-ph.SR]

work page arXiv 2025
[25]

de Jager, H

C. de Jager, H. Nieuwenhuijzen, and K. A. van der Hucht, Mass loss rates in the Hertzsprung-Russell dia- gram., A&AS72, 259 (1988)

1988
[26]

E. R. Beasor, B. Davies, N. Smith, J. T. van Loon, R. D. Gehrz, and D. F. Figer, A new mass-loss rate pre- scription for red supergiants, MNRAS492, 5994 (2020), arXiv:2001.07222 [astro-ph.SR]

work page arXiv 2020
[27]

Freytag, H

B. Freytag, H. G. Ludwig, and M. Steffen, Hydrodynam- ical models of stellar convection. The role of overshoot in DA white dwarfs, A-type stars, and the Sun., A&A313, 497 (1996)

1996
[28]

Herwig, The evolution of AGB stars with con- vective overshoot, A&A360, 952 (2000), arXiv:astro- ph/0007139 [astro-ph]

F. Herwig, The evolution of AGB stars with con- vective overshoot, A&A360, 952 (2000), arXiv:astro- ph/0007139 [astro-ph]

work page arXiv 2000
[29]

Temaj, F

D. Temaj, F. R. N. Schneider, E. Laplace, D. Wei, and P. Podsiadlowski, Convective-core overshooting and the final fate of massive stars, A&A682, A123 (2024), arXiv:2311.05701 [astro-ph.SR]

work page arXiv 2024
[30]

Schroder, O

K.-P. Schroder, O. R. Pols, and P. P. Eggleton, A critical test of stellar evolution and convective core ‘overshooting’ 16 by means of zeta Aurigae systems, MNRAS285, 696 (1997)

1997
[31]

E. R. Higgins and J. S. Vink, Massive star evolution: rotation, winds, and overshooting vectors in the mass- luminosity plane. I. A calibrated grid of rotating single star models, A&A622, A50 (2019), arXiv:1811.12190 [astro-ph.SR]

work page arXiv 2019
[32]

E. E. Whitehead, R. Hirschi, V. Varma, B. Mueller, F. Rizzuti, C. Georgy, and W. D. Arnett, The impact of initial mass dependent convective boundary mixing on the structure and fates of massive stars, MNRAS546, staf2245 (2026), arXiv:2512.11728 [astro-ph.SR]

work page arXiv 2026
[33]

Davis, S

A. Davis, S. Jones, and F. Herwig, Convective boundary mixing in a post-He core burning massive star model, MNRAS484, 3921 (2019), arXiv:1712.00114 [astro- ph.SR]

work page arXiv 2019
[34]

Paxton, L

B. Paxton, L. Bildsten, A. Dotter, F. Herwig, P. Lesaf- fre, and F. Timmes, Modules for experiments in stellar astrophysics (mesa), The Astrophysical Journal Supple- ment Series192, 3 (2010)

2010
[35]

Farmer, C

R. Farmer, C. E. Fields, I. Petermann, L. Dessart, M. Cantiello, B. Paxton, and F. X. Timmes, On varia- tions of pre-supernova model properties, The Astrophys- ical Journal Supplement Series227, 22 (2016)

2016
[36]

C. E. Fields, The three-dimensional collapse of a rapidly rotating 16 msun star, The Astrophysical Journal Letters 924, L15 (2022)

2022
[37]

Andrassy, F

R. Andrassy, F. Herwig, P. Woodward, and C. Ritter, 3D hydrodynamic simulations of C ingestion into a convec- tive O shell, MNRAS491, 972 (2020), arXiv:1808.04014 [astro-ph.SR]

work page arXiv 2020
[38]

Renzo, J

M. Renzo, J. A. Goldberg, A. Grichener, O. Gottlieb, and M. Cantiello, Progenitor Stars Calculated with Small Re- action Networks should not be Used as Initial Conditions for Core Collapse, Research Notes of the American Astro- nomical Society8, 152 (2024), arXiv:2406.02590 [astro- ph.SR]

work page arXiv 2024
[39]

Grichener, M

A. Grichener, M. Renzo, W. E. Kerzendorf, R. Farmer, S. E. de Mink, E. P. Bellinger, C.-k. Chan, N. Chen, E. Farag, and S. Justham, Nuclear Neural Networks: Emulating Late Burning Stages in Core-collapse Super- nova Progenitors, ApJS279, 49 (2025), arXiv:2503.00115 [astro-ph.SR]

work page arXiv 2025
[40]

Farmer, C

R. Farmer, C. E. Fields, I. Petermann, L. Dessart, M. Cantiello, B. Paxton, and F. X. Timmes, On Vari- ations Of Pre-supernova Model Properties, ApJ227, 22 (2016), arXiv:1611.01207 [astro-ph.SR]

work page arXiv 2016
[41]

Grichener, A., Bug in the nuclear reaction rates of reactions with more than two reactants and/or products,https://github.com/MESAHub/mesa/issues/ 575(2023), mESAHub/mesa Issue #575

2023
[42]

com/MESAHub/mesa/pull/632(2024), mESAHub/mesa Pull Request #632

Farag, E., Fix rates detailed balance,https://github. com/MESAHub/mesa/pull/632(2024), mESAHub/mesa Pull Request #632. Merged: 2024-05-06. Accessed: 2026- 01-24

2024
[43]

The chemical composition of the Sun

M. Asplund, N. Grevesse, A. J. Sauval, and P. Scott, The Chemical Composition of the Sun, ARA&A47, 481 (2009), arXiv:0909.0948 [astro-ph.SR]

work page Pith review arXiv 2009
[44]

A. S. Jermyn, E. B. Bauer, J. Schwab, R. Farmer, W. H. Ball, E. P. Bellinger, A. Dotter, M. Joyce, P. Marchant, J. S. G. Mombarg, W. M. Wolf, T. L. Sunny Wong, G. C. Cinquegrana, E. Farrell, R. Smolec, A. Thoul, M. Cantiello, F. Herwig, O. Toloza, L. Bildsten, R. H. D. Townsend, and F. X. Timmes, Modules for Experiments in Stellar Astrophysics (MESA): Tim...

work page arXiv 2023
[45]

E. H. Anders and M. G. Pedersen, Convective Bound- ary Mixing in Main-Sequence Stars: Theory and Empiri- cal Constraints, Galaxies11, 56 (2023), arXiv:2303.12099 [astro-ph.SR]

work page arXiv 2023
[46]

Brott, S

I. Brott, S. E. de Mink, M. Cantiello, N. Langer, A. de Koter, C. J. Evans, I. Hunter, C. Trundle, and J. S. Vink, Rotating massive main-sequence stars. I. Grids of evolu- tionary models and isochrones, A&A530, A115 (2011), arXiv:1102.0530 [astro-ph.SR]

work page arXiv 2011
[47]

2013, ApJS, 208, 4, doi: 10.1088/0067-0049/208/1/4 10

B. Paxton, M. Cantiello, P. Arras, L. Bildsten, E. F. Brown, A. Dotter, C. Mankovich, M. H. Montgomery, D. Stello, F. X. Timmes, and R. Townsend, Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars, ApJS208, 4 (2013), arXiv:1301.0319 [astro-ph.SR]

work page internal anchor Pith review arXiv 2013
[48]

Vink, Jorick S., de Koter, A., and Lamers, H. J. G. L. M., Mass-loss predictions for o and b stars as a function of metallicity, A&A369, 574 (2001)

2001
[49]

J. Puls, J. S. Vink, and F. Najarro, Mass loss from hot massive stars, A&A Rev.16, 209 (2008), arXiv:0811.0487 [astro-ph]

work page arXiv 2008
[50]

Smith, Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars, ARA&A52, 487 (2014), arXiv:1402.1237 [astro-ph.SR]

N. Smith, Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars, ARA&A52, 487 (2014), arXiv:1402.1237 [astro-ph.SR]

work page arXiv 2014
[51]

K. M. Patton, C. Lunardini, and R. J. Farmer, Presu- pernova Neutrinos: Realistic Emissivities from Stellar Evolution, ApJ840, 2 (2017), arXiv:1511.02820 [astro- ph.SR]

work page arXiv 2017
[52]

C. Kato, H. Nagakura, S. Furusawa, K. Takahashi, H. Umeda, T. Yoshida, K. Ishidoshiro, and S. Yamada, Neutrino Emissions in All Flavors up to the Pre-bounce of Massive Stars and the Possibility of Their Detections, ApJ848, 48 (2017), arXiv:1704.05480 [astro-ph.HE]

work page arXiv 2017
[53]

Langanke, G

K. Langanke, G. Mart´ ınez-Pinedo, and J. M. Sam- paio, Neutrino spectra from stellar electron capture, Phys. Rev. C64, 055801 (2001), arXiv:nucl-th/0101039 [nucl-th]

work page arXiv 2001
[54]

T. Oda, M. Hino, K. Muto, M. Takahara, and K. Sato, Rate tables for the weak processes of sd-shell nuclei in stellar matter, Atomic Data and Nuclear Data Tables 56, 231 (1994)

1994
[55]

G. M. Fuller, W. A. Fowler, and M. J. Newman, Stellar weak-interaction rates for sd-shell nuclei. I - Nuclear ma- trix element systematics with application to Al-26 and selected nuclei of importance to the supernova problem, Astrophysical Journals42, 447 (1980)

1980
[56]

G. M. Fuller, W. A. Fowler, and M. J. Newman, Stellar weak interaction rates for intermediate-mass nuclei. II - A = 21 to A = 60, ApJ252, 715 (1982)

1982
[57]

G. M. Fuller, W. A. Fowler, and M. J. Newman, Stellar weak interaction rates for intermediate mass nuclei. III - Rate tables for the free nucleons and nuclei with A = 21 to A = 60, Astrophysical Journals48, 279 (1982)

1982
[58]

G. M. Fuller, W. A. Fowler, and M. J. Newman, Stel- lar weak interaction rates for intermediate-mass nuclei. IV - Interpolation procedures for rapidly varying lepton capture rates using effective log (ft)-values, ApJ293, 1 (1985)

1985
[59]

A. A. Dzhioev, A. V. Yudin, N. V. Dunina-Barkovskaya, A. I. Vdovin, A. A. Dzhioev, A. V. Yudin, N. V. Dunina- 17 Barkovskaya, and A. I. Vdovin, Neutrino Spectrum and Energy Loss Rates Due to Weak Processes on Hot 56Fe in Pre-Supernova Environment, Particles6, 682 (2023), company: Multidisciplinary Digital Publishing Institute Distributor: Multidisciplinar...

2023
[60]

A. A. Dzhioev, A. V. Yudin, N. V. Dunina-Barkovskaya, and A. I. Vdovin, Neutrinos from pre-supernova in the framework of TQRPA method, MNRAS527, 7701 (2023), arXiv:2312.07988 [nucl-th]

work page arXiv 2023
[61]

A. A. Dzhioev, A. V. Yudin, N. V. Dunina-Barkovskaya, and A. I. Vdovin, Neutrinos from pre-supernova: Effects of nuclear temperature on luminosities and spectra, Int. J. Mod. Phys. E33, 2441014 (2024)

2024
[62]

A. A. Dzhioev, A. V. Yudin, N. V. Dunina-Barkovskaya, and A. I. Vdovin, Pre-Supernova (Anti)Neutrino Emis- sion Due to Weak-Interaction Reactions with Hot Nuclei, Particles8, 84 (2025), arXiv:2512.21604 [nucl-th]

work page arXiv 2025
[63]

Misiaszek, A

M. Misiaszek, A. Odrzywolek, and M. Kutschera, Neu- trino spectrum from the pair-annihilation process in the hot stellar plasma, Phys. Rev. D74, 043006 (2006)

2006
[64]

2014, X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue, A&A, 564, A125, doi:10.1051/0004-6361/201322971

J. Buchner, A. Georgakakis, K. Nandra, L. Hsu, C. Rangel, M. Brightman, A. Merloni, M. Salvato, J. Donley, and D. Kocevski, X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue, A&A564, A125 (2014), arXiv:1402.0004 [astro-ph.HE]

work page internal anchor Pith review arXiv 2014
[65]

E. E. Whitehead, R. Hirschi, V. Varma, B. Mueller, F. Rizzuti, C. Georgy, and W. D. Arnett, The Impact of Initial Mass Dependent Convective Boundary Mixing on the Structure and Fates of Massive Stars, MNRAS 10.1093/mnras/staf2245 (2026), arXiv:2512.11728 [astro- ph.SR]

work page doi:10.1093/mnras/staf2245 2026
[66]

Iliadis,Nuclear physics of stars(2015)

C. Iliadis,Nuclear physics of stars(2015)

2015
[67]

O’Connor and C

E. O’Connor and C. D. Ott, Black Hole Formation in Failing Core-Collapse Supernovae, ApJ730, 70 (2011), arXiv:1010.5550 [astro-ph.HE]

work page arXiv 2011
[68]

Boccioli, D

L. Boccioli, D. Vartanyan, E. P. O’Connor, and D. Kasen, Neutrino Heating in 1D, 2D, and 3D core- collapse supernovae: characterizing the explosion of high- compactness stars, arXiv e-prints , arXiv:2501.06784 (2025), arXiv:2501.06784 [astro-ph.HE]

work page arXiv 2025
[69]

Horiuchi, K

S. Horiuchi, K. Nakamura, T. Takiwaki, and K. Kotake, Estimating the core compactness of massive stars with Galactic supernova neutrinos, Journal of Physics G Nu- clear Physics44, 114001 (2017), arXiv:1708.08513 [astro- ph.HE]

work page arXiv 2017
[70]

Segerlund, E

M. Segerlund, E. O’Sullivan, and E. O’Connor, Measur- ing the distance and mass of galactic core-collapse super- novae using neutrinos, arXiv e-prints , arXiv:2101.10624 (2021), arXiv:2101.10624 [astro-ph.HE]

work page arXiv 2021
[71]

arXiv e-prints , keywords =

E. Laplace, F. R. N. Schneider, and P. Podsiadlowski, It’s written in the massive stars: The role of stellar physics in the formation of black holes, A&A695, A71 (2025), arXiv:2409.02058 [astro-ph.SR]

work page arXiv 2025
[72]

Sukhbold and S

T. Sukhbold and S. E. Woosley, The Compactness of Presupernova Stellar Cores, ApJ783, 10 (2014), arXiv:1311.6546 [astro-ph.SR]

work page arXiv 2014
[73]

Griffiths, M.- ´A

A. Griffiths, M.- ´A. Aloy, R. Hirschi, M. Reichert, M. Obergaulinger, E. E. Whitehead, S. Martinet, L. Scia- rini, S. Ekstr¨ om, and G. Meynet, Evolving massive stars to core collapse with GENEC: Extension of equation of state, opacities and effective nuclear network, A&A693, A93 (2025), arXiv:2408.03368 [astro-ph.SR]

work page arXiv 2025
[74]

Chieffi and M

A. Chieffi and M. Limongi, The Presupernova Core Mass-Radius Relation of Massive Stars: Understand- ing Its Formation and Evolution, ApJ890, 43 (2020), arXiv:1911.08988 [astro-ph.SR]

work page arXiv 2020
[75]

C. Kato, R. Hirai, and H. Nagakura, The sensitivity of presupernova neutrinos to stellar evolution models, MN- RAS496, 3961 (2020), arXiv:2005.03124 [astro-ph.HE]

work page arXiv 2020
[76]

C. Kato, M. D. Azari, S. Yamada, K. Taka- hashi, H. Umeda, T. Yoshida, and K. Ishidoshiro, PRE-SUPERNOVA NEUTRINO EMISSIONS FROM ONe CORES IN THE PROGENITORS OF CORE- COLLAPSE SUPERNOVAE: ARE THEY DISTIN- GUISHABLE FROM THOSE OF Fe CORES?, The As- trophysical Journal808, 168 (2015), publisher: The American Astronomical Society

2015
[77]

Yoshida, K

T. Yoshida, K. Takahashi, H. Umeda, and K. Ishidoshiro, Presupernova neutrino events relating to the final evolu- tion of massive stars, Phys. Rev. D93, 123012 (2016), arXiv:1606.04915 [astro-ph]

work page arXiv 2016
[78]

C. Kato, H. Nagakura, A. Ito, R. Hirai, S. Furusawa, T. Yoshida, and R. Akaho, Comprehensive neutrino light curves and spectra: from pre-supernova evolution to early supernova phase, arXiv e-prints , arXiv:2603.09810 (2026), arXiv:2603.09810 [astro-ph.HE]

work page arXiv 2026
[79]

A. L. Baxter, S. Benzvi, J. C. Jaimes, A. Coleiro, M. C. Molla, D. Dornic, T. Goldhagen, A. Graf, S. Gris- wold, A. Habig, R. Hill, S. Horiuchi, J. P. Kneller, R. F. Lang, M. Lincetto, J. Migenda, K. Nakamura, E. O’Connor, A. Renshaw, K. Scholberg, C. Tunnell, N. Uberoi, A. Worlikar, and The Snews Collaboration, SNEWPY: A Data Pipeline from Supernova Simu...

2022
[80]

Hirschi, K

R. Hirschi, K. Goodman, G. Meynet, A. Maeder, S. Ek- str¨ om, P. Eggenberger, C. Georgy, Y. Sibony, N. Yusof, S. Martinet, V. Varma, and K. Nomoto, The fate of ro- tating massive stars across cosmic times, MNRAS543, 2796 (2025), arXiv:2508.21233 [astro-ph.SR]

work page arXiv 2025

Showing first 80 references.